//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11745 SUBJECT: OT 110215: NIR observations from NOT of GRB candidate DATE: 11/02/17 14:36:23 GMT FROM: Antonio Deugarte at IAA-CSIC A. de Ugarte Postigo, J.P.U. Fynbo, G. Leloudas, S. Geier, A. Man (DARK/NBI) P. Jakobsson (U. Iceland) report on behalf of a larger collaboration: We have observed the field of the optical transient OT 110215 (Sergey et al., GCNC 11739) using NOTCam at the 2.5m NOT telescope at Roque de los Muchachos Observatory (La Palma, Spain). Observations consisted of K and J-band observations starting on 16 Feb at 20:22 UT. The source 2MASS J00264184+8324093 is clearly identified in the individual images. We obtain photometric values of K=15.20+/-0.15 and J=16.45+/-0.12 consistent with those of the 2MASS catalogue. This implies that either the OT is unrelated to this 2MASS source or it that it has already returned to its quiescent state. We note that within a radius of ~5" we detect a total of 4 sources in the J-band image. with the following coordinates (J2000.0 +/- 0.5") and magnitudes: 1: 00:26:42.07,+83:24:09.3 # J = 16.45+/-0.12 (2MASS J00264184+8324093) 2: 00:26:41.46,+83:24:15.4 # J = 20.33+/-0.15 3: 00:26:37.47,+83:24:13.6 # J = 19.95+/-0.12 4: 00:26:36.70,+83:24:08.2 # J = 19.49+/-0.12 At this moment we cannot state variability of any of the sources. The 3-sigma limiting magnitude of our J-band image is ~ 21.0. Further analysis is ongoing. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11746 SUBJECT: Swift XRT and UVOT Observations of OT 110215 DATE: 11/02/17 23:07:06 GMT FROM: Margaret Chester at PSU M. M. Chester (PSU), J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU), H. A. Krimm (GSFC/USRA), N. P. M. Kuin (MSSL-UCL), F. E. Marshall (NASA/GSFC), and D. M. Palmer (LANL) report on behalf of the Swift team: Swift began a target of opportunity observation of OT 110215 on February 16, 2011 at 20:00:13 UT, 26.2 hours after the first detection of the optical transient (Sergey and Denisenko, GCN Circ. 11739). Swift data for these observations utilize Target ID 31928. We report a weak detection in XRT of a source consistent with the position of the OT; we obtain UVOT upper limits at the OT's position, but note a weak feature in the v-band 3.5 arc sec away. At the time the transient was first detected, the source position was far outside the Swift/BAT field of view (148 degrees from the boresight) and close to the Earth's limb, making BAT insensitive to gamma-rays associated with the event. The transient was also out of the FoV during the rebrightening reported by Sergey and Denisenko (GCN Circ. 11739). We have analyzed 4.6 ks of XRT data spanning from T0+26.3 to T0+28.5 hr. The data are entirely in Photon Counting mode. We detect a source with 3.8-sigma confidence consistent with the coordinates of the OT, with a count rate of 1.8 (+/- 0.8) x 10^-3 counts per second. No other source is detected within 3' of the OT. There is insufficient data to determine whether the source is fading or to do a spectral analysis. However, we note that the six photons detected all have energies below 1.5 keV, suggestive of a very soft source that would be more consistent with a stellar flare than the afterglow of a GRB. The UVOT instrument observed the field of the optical transient starting 2011-02-16 at 20:02:57 UT, 26.3 hours after the start of the OT, and ending at 22:18:33 UT. Only upper limits are obtained at the reported position of the transient. We note a weak feature in the reddest filter (v) at RA = 00:26:38, DEC = +83:24:10.5 (J2000), 3.5 arc sec away. The 3-sigma upper limits are given below. The magnitudes are based on the UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627); they are not corrected for the Galactic extinction corresponding to a reddening of E_{B-V} = 0.166 mag (Schlegel et al., 1998, ApJS, 500, 525). Filter exposure(sec) magnitude v 383 >20.1 b 383 >20.3 u 383 >19.8 uvw1 766 >20.3 uvm2 1092 >20.9 uvw2 1534 >21.3 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11750 SUBJECT: OT 110215: Further NIR observations from NOT of the GRB candidate DATE: 11/02/18 15:51:09 GMT FROM: Antonio Deugarte at IAA-CSIC A. de Ugarte Postigo, J.P.U. Fynbo, G. Leloudas, S. Geier, A. Man (DARK/NBI) and P. Jakobsson (U. Iceland) report on behalf of a larger collaboration: We have reobserved the field of the optical transient OT 110215 (Sergey et al., GCNC 11739) using NOTCam at the 2.5m NOT telescope at Roque de los Muchachos Observatory (La Palma, Spain). We obtained J and K-band imaging on 17 Feb between 20:10 and 21:56 UT with a seeing of 0.6". The 4 sources described in our previous circular (de Ugarte Postigo et al., GCNC 11745) are detected with consistent magnitudes, showing no clear variability in any of them between the 2 epochs. We note that source 3 is extended, the rest being unresolved. We do not detect anything at the position of the UVOT source (Chester et al., GCNC 11746) down to a 3-sigma limit of J ~ 21.5. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11768 SUBJECT: No IPN GRB detected in conjunction with candidate GRB 110215 DATE: 11/02/24 18:39:38 GMT FROM: Kevin Hurley at UCBerkeley/SSL K. Hurley, on behalf of the IPN, V. Connaughton, M. Briggs, and C. Meegan, on behalf of the Fermi-GBM team, S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and T. Cline on behalf of the Konus-Wind team, A. von Kienlin and A. Rau, on behalf of the INTEGRAL SPI-ACS GRB team, D. M. Smith, R. P. Lin, J. McTiernan, R. Schwartz, C. Wigger, W. Hajdas, and A. Zehnder, on behalf of the RHESSI GRB team, J. Goldsten, on behalf of the MESSENGER NS GRB team, K. Yamaoka, M. Ohno, Y. Hanabata, Y. Fukazawa, T. Takahashi, M. Tashiro, Y. Terada, T. Murakami, and K. Makishima on behalf of the Suzaku WAM team, E. Costa, E. Del Monte, I. Donnarumma, Y. Evangelista, M. Feroci, I. Lapshov, F. Lazzarotto, L. Pacciani, M. Rapisarda, P. Soffitta, for the SuperAGILE team, G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, M. Marisaldi, on behalf of the AGILE MCAL team, S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer, on behalf of the Swift-BAT team, and I. G. Mitrofanov, D. Golovin, M. L. Litvak, A. B. Sanin, W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on behalf of the Mars Odyssey GRB team, report: We have examined the data from 9 IPN spacecraft (RHESSI, Konus, INTEGRAL SPI-ACS, Swift BAT, MESSENGER, Mars Odyssey-HEND, Fermi GBM, Suzaku WAM, and AGILE) for evidence of a gamma-ray burst in conjunction with the optical transient associated with 2MASS J00264184+8324093 (GCN 11739). In most cases, the GRB-sensitive instruments were on, operating under good conditions, and the source was not Earth-blocked to them. There were two exceptions, however. There was a gap in the Mars Odyssey-HEND data which prevented the search for a response. Also, the position was far outside the Swift-BAT field of view (148 degrees from the boresight) and close to the Earth's limb, making BAT rather insensitive to gamma-rays from the source. The Fermi GBM was the most sensitive instrument; the source position was not occulted to Fermi by the Earth at the time of the OT, and several GBM detectors had a favorable geometry to the source position. No trigger or rate increase was detected around the time of the transient in any of the data. The most sensitive instruments in the IPN detect short duration bursts with fluences down to several times 10^-8 erg cm^-2 , and long duration bursts with fluences which are several times this value; thus we suggest that any burst associated with the transient must have had a fluence lower than ~3 x 10^-8 erg cm^-2, depending on its time history and energy spectrum.